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Heating and Dynamics of Two Flare Loop Systems Observed by AIA and EIS View all abstracts by submitter

Ying Li   Submitted: 2013-12-18 22:57

We investigate heating and evolution of flare loops in a C4.7 two-ribbon flare on 2011 February 13. From SDO/AIA imaging observations, we can identify two sets of loops. Hinode/EIS spectroscopic observations reveal blueshifts at the feet of both sets of loops. The evolution and dynamics of the two sets are quite different. The first set of loops exhibits blueshifts for about 25 minutes followed by redshifts, while the second set shows stronger blueshifts, which are maintained for about one hour. The UV 1600 observation by AIA also shows that the feet of the second set of loops brighten twice. These suggest that continuous heating may be present in the second set of loops. We use spatially resolved UV light curves to infer heating rates in the few tens of individual loops comprising the two loop systems. With these heating rates, we then compute plasma evolution in these loops with the ''enthalpy-based thermal evolution of loops'' (EBTEL) model. The results show that, for the first set of loops, the synthetic EUV light curves from the model compare favorably with the observed light curves in six AIA channels and eight EIS spectral lines, and the computed mean enthalpy flow velocities also agree with the Doppler shift measurements by EIS. For the second set of loops modeled with twice-heating, there are some discrepancies between modeled and observed EUV light curves in low-temperature bands, and the model does not fully produce the prolonged blueshift signatures as observed. We discuss possible causes for the discrepancies.

Authors: Y. Li, J. Qiu, M. D. Ding
Projects: SDO-AIA

Publication Status: Accepted for publication in ApJ
Last Modified: 2013-12-19 07:43
Go to main E-Print page  The behavior of transverse waves in nonuniform solar flux tubes. II. Implications for coronal loop seismology  Solar Cycle Variations of the Radio Brightness of the Solar Polar Regions as Observed by the Nobeyama Radioheliograph  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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